Formation of Cosmic structure : Theoretical ad obsoroational study

1.研究了星系的演化。我们（岛作和我）在Hogan、皮布尔斯和我（1996）提出的图像的基础上，建立了一个星系演化的定量模型。该模型再现了当时所有z < 1的观测结果，并被用作理解后来出现的更遥远星系的观测结果的基准。与这项工作有关，我们（MF，霍根和皮布尔斯）估计了宇宙中的重子预算，这将为理解重子平滑分布的宇宙结构的形成提供线索。从这项研究中得出的一个重要结论是，恒星中的重子数量很少，只有总丰度的1/4-1/10。基于冷暗物质的层次结构形成模型（MF和川崎，准备中），对这一小部分的理论理解也得到了推进。宇宙学参数的问题被重新讨论。在我们做的最多的工作中 ...更多信息 一个重要的方面涉及宇宙学距离尺度，特别是银河系内的距离尺度，这是任何河外距离尺度的第一步。我们（关口和MF）发现造父变星的PL关系包含令人惊讶的大金属丰度依赖，这将表明在估计到大麦哲伦云的距离时存在显著的误差。此外，我还回顾了随着Ilipparcos卫星的出现而变得明显的问题。事实上，lipparcos的结果给银河系内距离尺度的工作带来了比以往任何时候都多的混乱。我们现在正在研究与主序列拟合相关的不确定性问题。斯隆数字天空调查（SDSS）的工作仍在继续。我们已经为SDSS的测光部分的仪器工作了7年多，并使用1997年作为仪器的最后阶段。1998年5月，SDSS在测光仪器上看到了第一束光，随后的成像证实了设计的性能。随着仪器的完成，我们发表了一篇论文，描述了镶嵌CCD相机的技术和工程细节，我们认为这是天文学仪器的划时代成就。另一篇论文是为监视望远镜系统设计的高精度焦平面快门.我还研究了大质量中微子问题（MF，Tanimoto和Yanagida），这是由于超级神冈群的时间发现，以及QCD相变问题（与JLQCD合作），因为它们在宇宙学和宇宙起源学中的重要性。少

1. The evolution or galaxies is studied. We (Shimasaku and I) have constructed a quantitative model of galaxy evolution based on the picture advocated by Hogan, Peebles and myself (1996). The model reproduced all observations for z < 1 available at that time, and has since been used as a fiducial to understand the observations appeared later on for more distant galaxies. In connection to this work we (MF, Hogan and Peebles) have estimated the baryon budget in the universe, which should give a clue to understanding the formation of cosmic structure from smooth distributions of baryons. One important conclusion from this study is that the baryons in the stars arc a small amount, only 1/4-1/10 or the total abundance. Theoretical understanding as to this small fraction is also advanced in terms of a hierarchical structure formation model based on the cold dark matter (MF and Kawasaki, in preparation).2. The problem of the cosmological parameters is revisited. Among the work we did the most … More important aspect concerns the cosmological distance scales, in particular the distance scale within the Milky Way, which is the first step to any extragalactic distance scale. We (Sekiguchi and MF) found that the Cepheid PL relation contains surprisingly large metallicity dependence, which would indicate a significant errors involved in the estimate of the distance to Large Magellanic Cloud. In addition, I reviewed the problems which have been made clear with the advent of the Ilipparcos satellite. In fact the results of llipparcos have brought more confusions than ever into the work of the distance scale within the Milky Way. We are now studying the problem of uncertainties associated with the main sequence fitting.3. Work has continued for the Sloan Digital Sky Survey (SDSS). We have worked for the instrumentation for the photometric part of the SDSS for more than 7 years, and used the year 1997 for the final stage of the instrumentation. In May 1998 the SDSS saw the First Light on the photometric instrument, and the imagings that followed the First Light confirmed the designed performance. With the completion of the instrumentation we have published a paper describing the technical and engineering detail of the mosaic CCD camera, which we regard as an epoch-making achievement in the instrumentation for astronomy. Another paper is written for a high precision focal plane shutter for the Monitor Telescope system.4. I have also studied the problem or massive neutrinos (MF, Tanimoto and Yanagida), as motivated by time discovery of the Super-Kamiokande group, and the QCD phase transition issue (with JLQCD Collaboration) in view of their importance in cosmology and cosmogony. Less